While it was not the aim of this work to reproduce the nebular spectrum of
SN 2010lp exactly, we have shown that a density structure similar to that of
SN 1991bg, characterised by a low central density, reproduces the main features
of the observed spectrum. When the inner, \(^{56}\) Ni-rich region is replaced by an
oxygen-dominated mixture of lighter elements the [O i] emission seen in
SN 2010lp can be reproduced in overall intensity. A more exact match of the
double-peaked emission profile requires using two small blobs moving in opposite
directions at low velocity. The oxygen mass that is required to match the
emission line intensity is quite small, a total of \(\approx 0.04\)  \(\textrm {M}_{\odot }\) . There
is of course significant uncertainty on these values. Lacking a definitive
bolometric light curve[1]} present a preliminary
bolometric light curve of SN2010lp, but we do not know what reddening was used
and do not have the original photometry, which is still unpublished. we cannot
confidently estimate the overall \(^{56}\) Ni mass, which affects the excitation of
the central oxygen at late times. The lack of a nebular spectral series makes it
difficult to determine accurately the densities in the inner layers: the
changing ionization as a function of time is very important in this respect
[2]}, [3]}.
